This study focusses on the CTTS RU Lup, which is known to have a plethora of strong accretion features [1]}, [2]}, [3]}. RU Lup is an accreting CTTS of 2 – 3 Myrs that lies in the Lupus star-forming region at a distance of \(d\approx 159\)  pc [4]}. It has a rotational period of \(3.71\pm 0.01\)  [5]} and is notable for its strong emission lines and veiling. These accretion-tracing lines are exceptionally broad, for example, the equivalent width (EW) of the H\(\alpha \)  emission line is usually found to be greater than 100 Å [3]}. In their models, this high accretion activity was found by [7]} to be responsible for the majority of the observed luminosity, whereby only about 10% is generated by gravitational contraction of the star itself. The \(\dot{M}_{\text{\,acc}}\)  was calculated by [8]} and found to be \(\sim \!1.8\times 10^{-8}\)  \(M_{\odot }\) yr\(^{-1}\) . The study by [9]} resulted in values of \(\sim \!6.7\times 10^{-8}\)  \(M_{\odot }\) yr\(^{-1}\) . This spread is indicative of the amount of accretion variability exhibited in RU Lup on the timescales of years. For this study we measured the \(\dot{M}_{\text{\,acc}}\)  of RU Lup during 2011 and determined how it changes over the shorter timescale of two weeks. By investigating its short-time stellar-disk magnetospheric interaction, our dataset allowed the exploration of how RU Lup's accretion fits into the category of routine variability, as delineated in Table 1. of [10]}.
